The Proposed Holographic Noise Experiment Rainer Weiss , MIT On behalf of the proposing group Fermi Lab Proposal Review November 3, 2009

Strategy for the Experiment Direct test for the holographic noise Positive signal if it exists Sufficient sensitivity Provide margin for prediction Probe systematics of perturbing noise Measure properties of the holographic noise Frequency spectrum Spatial correlation function

Experiment Concept Measurement of the correlated optical phase fluctuations in a pair of isolated but collocated power recycled Michelson interferometers exploit the spatial correlation of the holographic noise use the broad band nature of the noise to measure at high frequencies where other correlated noise is expected to be small

Pedagogic Michelson Interferometer

Schematic of Power Recycled Michelson PBS ~ P0 / ifo loss S. Waldman

Experiment parameters Input laser power @ 1.06 m 0.75 watt Arm length BS - EM 40 meters Free spectral range recycling cavity 3.5 MHz Min. beam waist diameter 7.4 mm Power recycling arm length 0.5 meter End mirror transmission 10ppm Beam splitter transmission 0.5 Anti reflection coating reflectivity 10 ppm Mirror loss (PRM,BS,TM) 50 ppm Substrate loss Differential arm loss 25 ppm Power on BS 2 kW Differential length offset 4 x 10-10 meters = 4 x 10-4 l Output power at antisym 10 mW 5mW / detector Recycling mirror transmission 1.0x10-3 Recycling cavity frequency pole 365 Hz Transimpedance of preamp 100 ohms Preamp voltage noise 3nV/sqrt(Hz) Quantum phase noise 9 x 10-12 radians/sqrt(Hz)

Basic experiment relations signal quantum phase fluctuations: expected dominant noise

Basic experiment relations Interferometer correlation

Transfer functions for differential and common mode loops S. Waldman

S. Waldman

S. Waldman

S. Waldman

S. Waldman

Noise sources Preamplifier voltage and Johnson Noise Poisson noise due to reduced contrast Unbalance end mirror reflectivities Overlap of beams at BS rms longitudinal motion Gdiff~ 105 B ~ 10kHz

Noise sources Phase noise from amplitude fluctuations Phase noise from frequency noise Not serious Phase noise from scattering paths

Noise sources Phase noise from forward scattering by the residual gas P < 10-4 lower pressure to avoid mirror contamination

Comparison of phase noise Interferometer Power on beam splitter watts Phase noise rad/sqrt(Hz) LIGO Phase noise interferometer (1998) 70 3 x 10-10 LIGO H1,L1 (2009) 250 2 x 10-11 GEO 600 (2009) 2700 8 x 10-12 /SRGain Proposed instrument 2000 9 x 10-12 @ f > 10kHz

LIGO Phase Noise Test Interferometer

About the optics All optics requirements can be met by (now) standard superpolish surfaces coated by plasma thin film deposition. To avoid thermal lensing in the beam splitter will need to use low loss Heraeus fused silica such as Supersil 3001/3002/300. Purchase dedicated coating runs with commercial vendor for initial components and spares. Use vacuum compatible PZT controlled 2” optics mounts being developed in industry by the Advanced LIGO project.

Uncertainties and decisions to be made In vacuum or outside detectors begin with outside detectors, decide from initial noise performance PZT hard optics mounts or suspensions begin with PZT, decide from required locking dynamic range Alignment servos begin with simple adjustment, add dither servo alignment if needed Laser frequency stabilization and filtering begin with only interferometer common mode feedback to laser, add in-line filter cavity and active frequency stabilization to reference cavity if needed